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Optimising Spectroscopic and Photometric Galaxy Surveys: Same-Sky Benefits for Dark Energy and Modified Gravity

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Optimising Spectroscopic and Photometric Galaxy Surveys: Same-Sky Benefits for Dark Energy and Modified Gravity Mon. Not. R. Astron. Soc. 000, 1–21 (2009) Printed 12 September 2018 (MN LATEX style file v2.2) Optimising Spectroscopic and Photometric Galaxy Surveys: Same-sky Benefits for Dark Energy and Modified Gravity Donnacha Kirk1, Ofer Lahav1, Sarah Bridle2, Stephanie Jouvel3, Filipe B. Abdalla1, Joshua A. Frieman4 1Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK 2Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK 3Institut de Ci`encies de l’Espai (ICE, IEEC/CSIC), E-08193 Bellaterra (Barcelona), Spain 4Fermilab Center for Particle Astrophysics, Batavia, IL 60510 4Kavli Institute for Cosmological Physics, The University of Chicago, Chicago, IL 60637 12 September 2018 ABSTRACT The combination of multiple cosmological probes can produce measurements of cosmo- logical parameters much more stringent than those possible with any individual probe. We examine the combination of two highly correlated probes of late-time structure growth: (i) weak gravitational lensing from a survey with photometric redshifts and (ii) galaxy clustering and redshift space distortions from a survey with spectroscopic redshifts. We choose generic survey designs so that our results are applicable to a range of current and future photometric redshift (e.g. KiDS, DES, HSC, Euclid) and spectroscopic redshift (e.g. DESI, 4MOST, Sumire) surveys. Combining the surveys greatly improves their power to measure both dark energy and modified gravity. An independent, non-overlapping combination sees a dark energy figure of merit more than 4 times larger than that produced by either survey alone. The powerful syner- gies between the surveys are strongest for modified gravity, where their constraints are orthogonal, producing a non-overlapping joint figure of merit nearly 2 orders of magnitude larger than either alone. Our projected angular power spectrum formal- ism makes it easy to model the cross-correlation observable when the surveys overlap on the sky, producing a joint data vector and full covariance matrix. We calculate a same-sky improvement factor, from the inclusion of these cross-correlations, relative to non-overlapping surveys. We find nearly a factor of 4 for dark energy and more than a factor of 2 for modified gravity. The exact forecast figures of merit and same-sky benefits can be radically affected by a range of forecasts assumption, which we explore methodically in a sensitivity analysis. We show that that our fiducial assumptions arXiv:1307.8062v1 [astro-ph.CO] 30 Jul 2013 produce robust results which give a good average picture of the science return from combining photometric and spectroscopic surveys. Key words: cosmology: observations – gravitational lensing – dark energy – modified gravity – cosmological parameters – large-scale structure of Universe 1 INTRODUCTION Colless 2003) chronicle the growth of cosmic structure and Weak Gravitational Lensing (WGL) (Hoekstra & Jain 2008; The era of “precision cosmology” is now a reality. Different Heymans 2012) gives us, through the bending of light, ac- cosmological probes are able to measure some of the most cess to dark matter, the dominant matter species, invisible fundamental properties of our Universe from the Cosmic to direct observation. Microwave Background (CMB) (Planck Collaboration et al. The next decade will bring an even greater wave of 2013; Carlstrom 2011; Sievers 2013) to the type Ia su- data as many of these cosmic probes are scaled up to pernovae (SNe) (Riess 1998; Perlmutter 1999) which chart cover more area on the sky, greater volumes and more ob- the accelerating expansion of the Universe. Large volume jects. We detail a number of these surveys in tables 1 and surveys of galaxies and galaxy clusters (Eisenstein 2005; 2 (Soares-Santos & DES Collaboration 2012; Amiaux 2012; c 2009 RAS 2 Donnacha Kirk, Ofer Lahav, Sarah Bridle, Stephanie Jouvel, Filipe B. Abdalla, Joshua A. Frieman Abdalla 2012; de Jong 2012; Pilachowski 2012; Sugai 2012a). ing RSDs) from the spectroscopic redshift (spec-z) survey. Each probe of cosmology requires an enormous effort to un- This pared down approach allows us to explore the impact derstand both the underlying physics and subtle systematic of nuisance parameter modeling & choice, survey strategy and observational effects as well as the creation of innovative and survey overlap in a clean way without having to deal new statistical techniques to deal with the sheer quantity of with too many competing effects. For the same reason we data being produced. In engineering terms these projects are choose to model both probes and their cross-correlations in often pushing boundaries in terms of space science, optics, the same projected angular power spectrum formalism. detector design, computation and data storage. Cosmologi- The combination of a photo-z WGL survey and a spec-z cal probes are generally complementary, in that each probes galaxy clustering survey has been studied by a number of a different combination of the cosmological parameters we papers including Cai & Bernstein (2012); Gazta˜naga et al. are interested in, while being sensitive to different sets of (2012); Duncan et al. (2013); de Putter et al. (2013). In gen- nuisance parameters and systematics. eral these papers have modelled different observables us- While each different cosmological probe will gather data ing different formalisms. Our approach in this paper is to of unprecedented precision over the next decade and be- model both WGL and galaxy clustering, including RSDs as yond, it is already clear that the strongest constraints on projected angular power spectra, C(l) (Hu 1999; Bernstein cosmology come from the proper combination of different 2009). While there may be some loss in accuracy for the probes (Kilbinger 2013; Jee et al. 2013). These combinations spec-z case due to projection along redshift we are inter- break degeneracies between cosmological (and nuisance) pa- ested in presenting a unified framework in which each ob- rameters and allow a level of precision much beyond any servable is treated on the same footing and cross-correlations individual probe. Indeed this is the source of our current can be handled naturally. This fits with the philosophy of “concordance cosmology”, ΛCDM (Komatsu 2011). Some jointly modelling all cosmological/systematic effects in the cosmological probes are relatively independent, perhaps the same ‘combined probes’ data vector and a single joint co- CMB and SNe are a good example. These probes can be variance matrix. In the same spirit we try to make explicit combined in a very simple way without worrying about the all assumptions about observable/survey modelling and the cross-talk between observables or double counting of infor- treatment of nuisance parameters. For the most fundamen- mation. This, however, is the exception. Most probes are tal assumptions we examine the impact of varying each in- highly correlated as they probe the same underlying phys- dependently as a sensitivity analysis. A full “optimisation” ical processes, whether that is the expansion history of the would vary these assumptions simultaneously and search for Universe or the perturbations of the large-scale gravitational the best combination but we think many are currently so potential as it evolves with time. ill-understood that it is more important to disentangle the Given this situation, increasing attention is being paid separate effects. Each assumption will require specialist at- to the correct way to combine multiple cosmological probes. tention to settle on a “correct” approach, we hope merely While the relatively independent probes we mentioned can to demonstrate the power of these assumptions to change be treated separately and combined on the level of multiplied survey results and the need for detailed further attention. posterior probabilities, this is not possible with the late- This paper forms a companion piece to Jouvel (2013). time Large-Scale Structure (LSS) probes which are highly We model similar surveys but, as a division of labour, we correlated both in terms of cosmological information and restrict consideration of target selection, survey design and in systematic effects. In these cases it is essential to con- observing strategy to Jouvel (2013). This paper considers struct a joint data vector which can model all cosmolog- assumptions on theoretical formalism, systematics includ- ical and systematic effects simultaneously, including their ing galaxy bias & photo-z error, survey overlap and more. cross-correlations, and avoid double counting. In addition Assumptions varied in Jouvel (2013) are fixed in this paper one should perform a simultaneous joint likelihood analysis and vice versa. using a covariance matrix which includes all cross correla- Section 2 talks about the landscape of photo-z and spec- tion terms (and off-diagonal elements) between the different z surveys. Then in section 3 we present our C(l)s formalism probes. If these complications are ignored the final result can for both cosmic shear and galaxy clustering before detail- be strongly biased (Eifler et al. 2013; Taylor et al. 2013). ing the rest of our assumptions about nuisance parameters For clarity this paper concentrates on the combination and fiducial survey strategies in section 4. Our forecast con- of two types of survey which will become available over straints on DE and MG are given in section 5, where each the next 5-10 years. We choose a large area optical cosmic subsection details the impact of a move away from our fidu- shear survey with photometric-quality redshifts, modelled cial assumptions. We draw together the implications of these on the Dark Energy Survey (DES) (5000 deg2 with 200 results in section 6 before concluding in section 7. ∼ million galaxies) and a medium scale spectroscopic LSS sur- vey (5000 deg2 targeting 10 million galaxies) similar to the ∼ DESI (combined Big-BOSS, DESpec), 4MOST and Sumire 2 PHOTOMETRY & SPECTROSCOPY concepts (Abdalla 2012; de Jong 2012; Pilachowski 2012; Sugai 2012a). See tables 1 and 2 for more details on cur- When we make a survey of galaxies in the Universe, rent and future surveys.
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